LISA: Opens the low-frequency gravita=onal universe ! 1 22 Years - PowerPoint PPT Presentation

LISA: Opens the low-frequency gravita=onal universe ! 1

22 Years aAer the First LISA Symposium at RAL 1996 2

LISA: A Mature Concept • M3 proposal for 4 S/C ESA/NASA collabora=ve mission in 1993 • LISA selected as ESA Cornerstone in 1995 • 3 S/C ESA/NASA LISA appears in 1997 • Joint ESA-NASA Mission Formula=on study 2005-2011 • Reformula=on 2012-13 as ESA-led eLISA (evolving LISA) • Now back to 3-arm LISA with NASA 3

But then in March 2011... 4

Then came 2015/2016.... • And two things happened! 5

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Black Holes every Month! Credit: LIGO/Caltech/Sonoma State (Aurore Simonnet) 7

LISA Pathfinder • Tes=ng LISA technology in space! 8

First Proposed in 1998 as ELITE • European LIsa TEchnology Satellite • Renamed to SMART-2 in 2000 – Tech demo for LISA and Darwin – Launch date 2006 • Descoped to LISA Pathfinder – Darwin demo cancelled 9

17 years later! September 2015: SpacecraA is completed! 10

100 Years since GR Publica=on: Dec. 2, 2015 11

P HYSICAL R EVIEW L ETTERS 10 J UNE 2016 Member Subscription Copy Articles published week ending Library or Other Institutional Use Prohibited Until 2017 Published by American Physical Society Volume 116, Number 23 12

Accelera=on Spectrum 10 -14 m/s 2 = 1 femto-g 1 hour 1 minute 1 sec 13

LISA Pathfinder shows: LISA Works! LISA Pathfinder Requirement LISA Requirement LISA Pathfinder Performance Feb 2017 14

ESA L2 and L3 Missions • Call for Mission Concepts fall 2016 15

NASA is back in LISA! 16

LISA Mission Concept Document • Submided on January 13th, 2017 • The LISA Consor=um: 12 EU Member States plus the US ! hdps://www.lisamission.org/proposal/LISA.pdf 17

Mission Profile and Orbit • Three arms of 2.5 Million km • 2W lasers • 30 cm telescopes • Breathing angles ± 1 deg • Doppler shiAs ± 5 MHz • Launch on dedicated Ariane 6.4 – Transfer =me ~400 days – Direct escape V ∞ = 260 m/s – Propulsion module and S/C composite 18

ESA Member State Involvement • Tradi=onally: – ESA: spacecraA bus – ESA member state agencies: science instrument • In old ESA/NASA LISA: – Payload was European contribu=on paid for by ESA – Different from other L1 mission candidates • In L3 LISA: – Use tradi=onal approach of na=onal consor=um 19

What is the instrument on LISA? • Treat like focal plane instrument for Astronomy mission • ESA responsible for: – Satellite plamorm, including: • Telescope, laser and structure for op=cal assembly moun=ng • Member States fund: – Scien=fic consor=um to deliver instrument consis=ng of: • Op=cal Bench with adached Iner=al Sensor and detached Phasemeter, Payload Computer 20

The Science Instrument • Provided by LISA Consor=um (D, F, I, UK, ES, CH, DK, NL, SE, PT, HU, RO) plus USA • Also provided LISA Pathfinder Instrument S/C mounted Gravita=onal Op=cal Bench (OB) Reference Sensor (GRS) DMU ULU PM www.lisamission.org FEE 21

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LISA Organigram in Phase A 23

ESA SPC selected LISA as L3 ! 24

Start of Phase 0: CDF Study 25

ESA and NASA are in it together! 26

ITT for LISA Phase A 27

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LISA Requirements 29

LISA Sources 30

LISA Pathfinder shows: LISA Works! LISA Pathfinder Requirement LISA Requirement LISA Pathfinder Performance Feb 2017 31

LISA for Astrophysics, Cosmology, and Fundamental Physics Massive Black Holes (10 4 to 10 8 M ☉ ) • When did the first Black Holes appear in pre-galac=c halos and what is their mass and spin? – How did Black Holes form, assemble and evolve from cosmic dawn to present =me, due to accre=on and mergers? – What role did Black Holes play in re-ionisa=on, galaxy evolu=on and structure forma=on? – What is the precise luminosity distance to loud standard siren black hole binaries? – What is the distance – redshiA rela=on and the evolu=on history of the universe? – Does the Graviton have mass? – Extreme Mass Ra=o Inspirals, EMRIs (1 to 10 M ☉ into 10 4 to 5 x 10 6 M ☉ ) • How is the stellar dynamics in dense galac=c nuclei? – How does dynamical relaxa=on and mass segrega=on work in dense galac=c nuclei? – What is the occupa=on frac=on of black holes in low-mass galaxies? – How large are devia=ons from Kerr Metric, and what new physics causes them? – Are there horizonless objects like boson stars or gravastars? – Are alterna=ves to GR viable, like Chern-Simons or scalar tensor theories or braneworld scenarios? – Ultra-Compact Binaries in Milky Way • What is the explosion mechanism of type Ia supernovae? – What is the forma=on and merger rate of compact binaries? – What is the endpoint of stellar evolu=on? – Stochas=c Signals • Directly probe Planck scale epoch at 1 TeV to 1000 TeV before decoupling of microwave background – Were there phase transi=ons and of which order? – Probe Higgs field self coupling and poten=al, and search for supersymmetry. – Are there warped sub-millimetre extra-dimensions? – Can we see braneworld scenarios with rehea=ng temperatures in the TeV range? – Do topological defects like Cosmic Strings exist? – The Unknown ! • ??? 32

Black Hole Astronomy by 2030 Redshift Z à ET (proposed) Future EM Obs. LSST, JWST, EELT SKA, Pulsar aLIGO, aVIRGO, Timing KAGRA Mass [log M/M ☉ ] à 33

Black Hole Astronomy by 2030 20 10 20 15 LISA 50 Redshift Z à 100 200 10 z 500 SNR 1000 5 0 10 2 10 3 10 4 10 5 10 6 10 7 10 8 10 9 10 10 M Mass [log M/M ☉ ] à 34

All Binary Black Holes cross LISA band: Trace Galaxy Mergers Time 35

Extreme Mass Ra=o Inspirals • SNR 20 up to z ≈ 0.7 for 10 5 -10 6 M ⊙ • Dozens of events per year • Mass, spin to 0.1% – 0.01 % • Quadrupole moment to < 0.001 M ⊙ 3 G 2 /c 4 • Do Black Holes have hair? – New objects in General Rela=vity • Boson Stars, Gravastars, non-Kerr solu=ons (e.g. Manko-Novikov) – Devia=ons from General Rela=vity • Chern-Simons, Scalar-Tensor, light scalar fields (axions) and black hole bomb instabili=es • Each has specific GW fingerprint! 36

Dark Mader Probe • Dark Mader spike around BH changes inspiral GW phase • Sensi=ve even to Dark Mader α interac=ng only gravita=onally ! $ r 0 ρ DM = ρ 0 # & " r % 37

Cosmology with Standard Sirens No identifications • With luminosity distances, LISA gives accurate and independent measurements of H 0 and w. § EMRIs, without EM counterparts: § Hubble const. H 0 to ±0.4% = ±0.3 km s -1 Mpc -1 aAer 20 EMRI detec=ons: ~3 months LISA (MacLeod & Hogan, PRD, 2008; SDSS) With identifications § Compare WMAP: ±1.2 km s -1 Mpc -1 . § MBH mergers out to z = 3, no EM counterparts: § Dark energy equa=on of state parameter w to ±2-4% in 3 years (Pe=teau et al, ApJ, 2011; Millennium). § Compare EUCLID: ±2%. Dark Energy equa=on-of-state parameter w

LISA Cosmology N. Tamanini 2017 39

The new LISA Data Challenge (LDC) • Resurrec=ng data challenges • Project hosted under git-lab: – hdps://gitlab.in2p3.fr/stas/MLDC (sign up is required) • Project oriented: – Each data set aims at par=cular data analysis problem • Ul=mate goal: – Build a robust data analysis pipeline for the LISA mission. • Web-page will be open shortly for everyone to sign up for the challenge and download the simulated data set.

LDC webpage

LISA: LIGO Event Predicted 10 Years in Advance! • Accurate to seconds and within a square-degree! GW150914 42

ESA L2 and L3 Missions • Call for Mission Concepts fall 2016 • Decision on L3 Adop=on 2021 • Launch of L2 in 2028 • Launch of L3 in 2034 • LISA shall be ready for an early launch! 43